Gamma-Ray Burst (GRB) Science with LST - UC Santa Cruzphysics.ucsc.edu/~joel/GRB2010/CTA_LST_ioka10.pdf · max ! Fireball expands by radiation pressure!! In principle, G max ~ Energy

Gamma-Ray Burst (GRB) Science !

with LST

Kunihito Ioka (KEK)!on behalf of the GRB subtask

CTA LST meeting 2010@RAL

•  !"#$%&'()&($*'+,$-./$–  -0*(1$2'3'+$0)$+,($4526$-01()+7$89&+01$

•  !:;<<<$'%$'3=01+9)+>$5%5922?$)0+$(@=$&5+0A>$)0+$)(&(%%91'2?$+,($%93($1(B'0)$

–  $C3'%%'0)$3(&,9)'%3D$9E(1B20*F=103=+G$-(=+0)H%?)GFIJGKF,9L10)G$

•  .=(&D$39@$%?)&,10>$IJ$&03=0)()+>$/(3=192D$M3(N1(%02O(L$•  -0)B$04%D$(912?$9E(1B20*>$C912?$04%D$!(P$0)%(+$L(29?$H*F$=1(&51%01K$

–  $Q104')B$C#->$R'B,N7D$-IPG$S@'0)G>$T'1%+$%+91>$I.U$#$–  $-IP$H*'+,$J/S$0)2?K$

•  #(%+$%&()91'0D$C)(1B?$'%$L03')9+(L$4?$/(P>$)0$&5+0A$-01()+7$89&+01:;<<<<>$P'029+($C#-$V$-IPW$V$IJCJX#CY!ZW

GRB Subtask

[email protected][email protected][email protected]

inaugurated Mar. 18, 2010

Ryde, Felix!Tam, P. H. Thomas!Teshima, Masahiro!Toma, Kenji!Torres, Diego!Wagner, Stefan!Wijers, Ralph!Yamazaki, Ryo!Zech, Andreas!

Asano, Katsuaki!Falcone, Abe!Granot, Jonathan (Yoni)!Hinton, Jim!Horns, Dieter!Inoue, Susumu!Inoue, Yoshiyuki!Ioka, Kunihito!Kakuwa, Jun!Lamanna, Giovanni!Markoff, Sera!Murase, Kohta!O’Brien, Paul!Raue, Martin!

You are welcome to join us

Red: Leaders

GRB: Brightest Explosion

=! = Sun~1033g!

GRB!~1052erg!Atomic bomb

In ~sec, GRB release energy Sun emit over lifetime!

GRB is the most luminous object

E=mc2 (by Einstein)"

~1kg!

GRB in a Nutshell

Photo-!sphere

Internal!Shock

External!Shock

Time

Flux

~2-100s!~0.01-2s

Relativistic Jet!G>100!

ISM

~2-3/day@Cosmological!Long: Massive Stellar!!Collapse to BH/NS!

Short: NS-NS/BH merger?!!Magnetar? Long GRB?

Ekin⇒Eg

AfterglowPrompt

GRB Spectrum

•  Band spectrum

MeV

Epeak

GeV TeVkeV

nFn

n

∝n

∝n-0.5

CTA

Fermi Revolution~30 GeV g from GRBs ⇒!

Guaranteed source for CTA

CTA

GRB 090510

Abdo+ 09!

GeVMeVkeV

Fermi GRB Features1. Extra spectral "

component2. Temporally "

Extended "Emission

t#1.2±0.2"

GRB 090510

up to >1000sec(But minor; majority is Band)

GRB080916CkeV MeV

GeV

Pre-Fermi Era

! EGRET!•  GRB940217 (Hurley+94)!

– 18GeV to 90min!

•  GRB941017 (Gonzalez+03)!– Temporary distinct HE!

! AGILE!•  GRB080514B (Giuliani+08)!

– Long-lived HE!

New Features

MeV

GeV

3. GeV onset delay

~1 sec

4. Photosphere-like

GRB 090902B

Abdo+ 09!

~ Black Body!(But minor)

Detections as of 090904 Detections as of 090904

GRB!Angle from LAT!

Duration!(or class)!

# of events > 100 MeV!

# of events > 1 GeV!

Delayed HE

onset!

Long-lived HE

emission!

Extra spectral comp.!

Highest photon Energy!

Redshift!

080825C! ~ 60°! long! ~ 10! 0! ?! ! X! ~ 600 MeV!

080916C! 49°! long! 145! 14! ! ! ?! ~ 13.2 GeV! ~ 4.35!

081024B! 21°! short! ~ 10! 2! ! ! ?! 3 GeV!

081215A! ~ 86°! long! —! —! —! —! --! —!

090217! ~ 34°! long! ~ 10! 0! X! X! X! ~ 1 GeV!

090323! ~ 55°! long! ~ 20! > 0! ?! ! ?! 3.57!

090328! ~ 64°! long! ~ 20! > 0! ?! ! ?! 0.736!

090510! ~ 14°! short! > 150! > 20! ! ! ! ~ 31 GeV! 0.903!

090626! ~ 15°! long! ~ 20! > 0! ?! ! ?!

090902B! 51°! long! > 200! > 30! ! ! ! ~ 33 GeV! 1.822!

090926! ~ 52°! long! > 150! > 50! ! ! ! ~ 20 GeV! 2.1062!

091003A! ~ 13°! long! ~ 20! > 0! ?! ?! ?! 0.8969!

091031! ~ 22°! long! ~ 20! > 0! ?! ?! ?! ~ 1.2 GeV!

100116A! ~ 29°! long! ~ 10! 3! ?! ?! ?! ~ 2.2 GeV!11 ©Ohno

~18 LAT+GMB (as of Jul 2010): No HE cutoff"

Exception

Spectral break @~1.4GeV!G~200-700 if break is due to gg

10 102 103 104 105 106

Eg (keV)

GRB 090926A

Abdo+ 10

Implication of LAT RateComparable to !estimates based !on extrapolated!BATSE GRBs!no HE excess "nor deficit"(But,"D. Kocevski"@GRB2010)"Band is OK"Extra com."is rare"Band+ 09

MAGIC

Aleksic+ 10

Albert+ 06

MAGIC is consistent with the Band extrapolation

LST sensitivity

Konrad Bernlöhr!@Zeuthen10

Low energy!(<200GeV)!sensitivity is !determined!by LST

More g than Fermi!  Huge Effective Area!

–  Fermi ~1m2 @>10GeV!–  CTA ~104m2 @30GeV!

!  Expected # of g!–  (0.1-1)g x (104m2/1m2) !

~ 103-104 g per GRB!": Great Advantage of CTA"

~Background (but >30s CL)!~10kHz data taking is necessary

!  Extragalactic Background Light + Sensitivity!– gGRB(100GeV) + gEBL(10eV) → e+ + e-!

Energy Threshold.()%'MO'+?$[914'+191?\

Signal!(Schematic)

Low Energy !Sensitivity is !CRUCIAL

S. Inoue’s talk !in this CTA meeting

Rough Event Rate

!  Fermi LAT(GeV)/GBM(MeV) ~ 0.1!–  ~1000/yr x (LAT/GBM) ~ 100/yr (Conservative)!

1.  GRB in the FOV" ~100/yr x (Duty 0.1) x (FOV 5deg2) ~ 0.03/yr"

2.  Follow-up"–  Extended GeV emission lasts for >1000 sec!

–  ~20 sec slews are enough!

~100/yr x (Duty 0.1) x (Zenith 0.1) ~ 1/yr"GRB subtask (J. Kakuwa) is refining the estimate

Alert for Follow-up

Swift!up to ~2015?

SVOM!~2015-?!(approved)

JANUS!~2016-?

Upcoming New WindowsHigh Energy n Gravitational Wave

IceCube, KM3Net

LIGO, Virgo, GEO, "LCGT, AIGO, LISA, "DECIGO/BBO

GRB Science with CTA

1.  TeV calorimetry!2.  Lower limit on the bulk Lorentz factor!3.  Emission mechanism!

–  Site? Leptonic(syn?/IC?)/Hadronic?!

4.  Cosmology!–  Probing EBL, B!

5.  Lorentz Invariance Violation (w/ CTA only)!

6.  …

1. TeV Calorimetry

nFn

Energetics may be determined by TeV g

Abdo+ 10

IC/Syn~ee/eB>1!

E>1052erg!⇒ NS origin!

2. Lower limit on bulk G

!  gg→e+e- (eth~MeV)!–  R~cDt ⇒ t~sTNg/4pR2≫1 (g-ray cannot escape)!

!  Relativistic"–  R~G2cDt!–  Blueshift!–  t~G2b-2~G-6!

!  G>103!"v>0.999999"c

Gmin

RedshiftBut see also Li 08, Granot+08, Bosnjak+09, Aoi+KI 10, Zou+10!

Conventional Gmax

!  Fireball expands by radiation pressure!!  In principle, Gmax ~ Energy / Mass!!  Mass↓Gmax↑… However,!

⇒ Transparent before G~Gmax

Paczynski 86!Goodman 86!Shemi & Piran 90!Meszaros & Rees!

Γmax =�

LσT

4πmpc3r0

�1/4

∼ 103L1/453 r−1/4

0,7

Matter

Radiation!escapes

gg→e+e- Annhilation Break

!  Most likely Break (not Cutoff)

Aoi+ 10, Li 08, !Granot+08, Bosnjak+09

Time/Space!integration!

smears!the cutoff!

High-statistical!data or!

Time-resolved!spectrum is !important

3. Emission Mechanism

Photo-!sphere

Internal!Shock

External!Shock

Time

Flux

~2-100s!~0.01-2s

Relativistic Jet!G>100!

ISM

Ekin⇒Eg

AfterglowPrompt

!  Site!!  Mechanism!

– Syn? BB? Hadronic?!

!  Composition!–  p? Poynting? g? Fe?

GeV Models•  External shock – long-lived, but not variable!

–  Synchrotron (adiabatic/radiative shock)!–  SSC!–  External Compton of prompt g!

•  Internal shock!–  Synchrotron (peak at MeV) – not extra comp.!–  SSC – no low energy excess!–  Hadronic – proton luminosity is too large!–  External Compton of cocoon/photospheric g –

May need fine tuning!–  Synchrotron (peak at GeV-TeV) w/ High G!

!"" ~ 20 GeV #103

$ % &

' ( )

2+ 2** +1

!  gg→e+e- annhilation break!

!  IC component!

!  Max. Synchrotron Energy (tacc=tcool)!

!  Max. Synchrotron Energy (tacc=tdyn)

Possible TeV Features

!maxcool = mec

2

"# ~ 500 GeV #

104

$ % &

' ( )

!maxdyn ~ 1 GeV "

6 #104

$ % &

' ( ) *6

KI 10

How to separate!these from EBL abs.?

EBL Y. Inoue+ 10

EBL has a large uncertainty!Probe of early star/galaxy formation

GRB 090423!@ z~8.2

Intergalactic B

z=10!B=10-15G!

Proga 95!Takahashi+ 10

TeV gOpt-UV

e±CMB

MeV g

DelayB

GeV g

Delay time!⇒ B!

But, could be!contaminated!by afterglow

-IP

Summary

Rondo+ arXiv:0907.0626

~18 LAT+GMB GRBs (as of Jul 2010)!No HE cutoff within the sensitivity!

Zhang+ 10

090902B

Abdo+ 09